Geology of the lunar regional dark mantle deposits as seen by Clementine UVVIS data

Details Geology of the lunar regional dark mantle deposits as seen by Clementine UVVIS data Geology of the lunar regional dark mantle deposits as seen by Clementine UVVIS data

Mar 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997lpi....28.1533w&link_type=abstract

Conference Paper, 28th Annual Lunar and Planetary Science Conference, p. 533.

Computer Science

Lunar Geology, Dark Matter, Lunar Mantle, Clementine Spacecraft, Ultraviolet Spectroscopy, Volcanoes, Satellite Imagery, Crystallization, Ejecta, Spatial Resolution, Mineral Deposits

Scientific paper

We have used calibrated Clementine UVVIS data to map the geology and analyze spectra from several regional Dark Mantle Deposits (DMD) on the moon, including Taurus-Littrow (TL), Rima Bode (RB), Sulpicius Gallus (SG), Aristarchus Plateau (AP), and Orientale (OR). Regional DMD formed from pyroclastic eruptions and are composed of either volcanic glasses or crystallized beads. Unlike smaller localized dark mantle deposits, like those in Alphonsus and Franklin craters, which are only a few kms in diameter and are produced from vulcanian eruptions, regional DMD cover tens of km and indicate higher volume fluxes and plume heights. The crystallinity of the volcanic beads in a DMD is a very useful parameter for determining the cooling rates within the volcanic plume, with glasses indicating high cooling rates in a low optical density plume. Telescopic spectral data of the deposits indicate that TL and RB are dominated by crystallized black beads, SG is an equal mixture of glasses and black beads, while AP is dominated by the glasses. More recent Clementine data of the OR deposit on the lunar farside has shown that it is composed of volcanic glasses similar to those in the AP deposit.

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